MOLECULAR OUTFLOWS FROM THE PROTOCLUSTER SERPENS SOUTH
MOLECULAR OUTFLOWS FROM THE PROTOCLUSTER SERPENS SOUTH
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DOI：
10.1088/0004-637x/737/2/56
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发表时间：
2011-05
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影响因子：
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通讯作者：
F. Nakamura;Kohji Sugitani;Y. Shimajiri;T. Tsukagoshi;A. Higuchi;S. Nishiyama;R. Kawabe;M. Takami;J. Karr;R. Gutermuth;G. Wilson
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作者：
F. Nakamura;Kohji Sugitani;Y. Shimajiri;T. Tsukagoshi;A. Higuchi;S. Nishiyama;R. Kawabe;M. Takami;J. Karr;R. Gutermuth;G. Wilson
我们展示了使用 ASTE 10 m 望远镜对附近嵌入式星团 Serpens South 进行 CO (J = 3–2) 和 HCO+ (J = 4–3) 测绘观测结果。我们的 CO (J = 3–2) 图显示，许多流出物都聚集在密集的簇形成团块中，这些团块可以被识别为 HCO+ 团块，大小为 ∼0.2 pc，质量为 ∼80 M☉。该团块包含几个大小为 ∼0.05 pc 的子碎片。通过将 CO (J = 3–2) 图与 AzTEC 在 ASTE 上拍摄的 1.1 mm 尘埃连续谱图像进行比较，我们发现流出瓣的空间范围有时与稠密气体的分布呈反相关，并且一些流出瓣明显与稠密气体发生碰撞。总流出质量、动量和能量估计分别为 0.6 M☉、8 M☉ km s−1 和 64 M☉ km2 s−2。流出引起的能量注入速率与团块中的湍流耗散速率相当，这意味着原恒星流出可以维持该区域的超音速湍流。总流出能量似乎只有团块引力能的 10% 左右。我们得出的结论是，当前的流出活动不足以破坏整个星团形成团块，因此恒星形成可能会持续几个或许多局部动力学时间。
We present the results of CO (J = 3–2) and HCO+ (J = 4–3) mapping observations toward a nearby embedded cluster, Serpens South, using the ASTE 10 m telescope. Our CO (J = 3–2) map reveals that many outflows are crowded in the dense cluster-forming clump that can be recognized as an HCO+ clump with a size of ∼0.2 pc and mass of ∼80 M☉. The clump contains several subfragments with sizes of ∼0.05 pc. By comparing the CO (J = 3–2) map with the 1.1 mm dust continuum image taken by AzTEC on ASTE, we find that the spatial extents of the outflow lobes are sometimes anti-correlated with the distribution of the dense gas, and some of the outflow lobes apparently collide with the dense gas. The total outflow mass, momentum, and energy are estimated to be 0.6 M☉, 8 M☉ km s−1, and 64 M☉ km2 s−2, respectively. The energy injection rate due to the outflows is comparable to the turbulence dissipation rate in the clump, implying that the protostellar outflows can maintain the supersonic turbulence in this region. The total outflow energy seems only about 10% of the clump gravitational energy. We conclude that the current outflow activity is not enough to destroy the whole cluster-forming clump, and therefore star formation is likely to continue for several or many local dynamical times.